Publisher Information: KTH, Nordic Institute for Theoretical Physics NORDITA INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy. INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy. Univ Bologna, Dipartimento Fis & Astron Augusto Righi, Via Gobetti 93 2, I-40129 Bologna, Italy. INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy. INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy.; Inst Astrofis Canarias IAC, E-38200 San Cristobal la Laguna, Spain.;Univ La Laguna ULL, Dept Astrofis, E-38206 San Cristobal la Laguna, Spain. Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00100 Rome, Italy. INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy. MDPI AG 2022
نبذة مختصرة : We discuss the evolution of stars through the asymptotic giant branch, focusing on the physical mechanisms potentially able to alter the surface chemical composition and on how changes in the chemistry of the external regions affect the physical properties of the star and the duration of this evolutionary phase. We focus on the differences between the evolution of low-mass stars, driven by the growth of the core mass and by the surface carbon enrichment, and that of their higher mass counterparts, which experience hot bottom burning. In the latter sources, the variation of the surface chemical composition reflects the equilibria of the proton capture nucleosynthesis experienced at the base of the convective envelope. The pollution expected from this class of stars is discussed, outlining the role of mass and metallicity on the chemical composition of the ejecta. To this aim, we considered evolutionary models of 0.7-8 M & ODOT; stars in a wide range of metallicities, extending from the ultra-metal-poor domain to super-solar chemistries.
QC 20220304
Processing Request
No Comments.